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tokens: and abundance of galaxies in the Spitzer Matching survey of the UltraVISTA ultra-deep Stripes (SMUVS) to understand the connection between galaxies and their host dark matter halos. SMUVS provides a unique combination of large area (∼0.66 square degrees of the COSMOS field) and unparalleled depth at 3.6 and 4.5 μ m. This, combined with the latest ultra-deep UltraVISTA data and other ancillary data in the COSMOS field, allows for precise photometric estimates of redshift and stellar mass and robust statistics from such a large catalog ( objects). As a result, our analysis is performed over an unprecedented redshift range () for volume-limited galaxy samples selected by stellar mass. To interpret the observed clustering, we use a well-established five-parameter halo model, although we fix the values of three of these parameters. Novel to our approach is the inclusion of the photometric redshift dispersion, , as a free parameter in the fitting procedure. This parameter is designed to encapsulate the effect of dispersion in the photometric redshifts used in our analysis and allows us to fully exploit the clustering information in our photometric galaxy catalog. This parameter is discussed in more detail in Appendix A . From our best-fit halo models we can derive a number of interesting quantities. The characteristic halo masses, and , are well constrained by our data and exhibit fairly tight linear relationships (in logarithmic space) with stellar mass. This is similar to what has been found in earlier studies with similar analyses (e.g., McCracken et al. 2015 ). The satellite fraction, i.e., the fraction of galaxies in a sample that do not sit at the center of the potential well of their halo, generally increases with cosmic time. This is in broad agreement with other studies in the literature and in line with expectations of hierarchical structure formation. The comoving correlation length, r 0 , [defined such that ], and large-scale effective galaxy bias, , show strong monotonic trends with increasing redshift for a fixed stellar mass over the entire redshift range probed. Projecting ΛCDM halo mass accretion histories computed according to Appendix A of McBride et al. ( 2009 ) through our measurements of the large-scale bias, and combining this with the evolution of stellar mass content based on the cumulative number density (Behroozi et al. 2013a ), we propose an evolutionary path for the dark matter and stellar mass content of galaxies for . This shows a favorable agreement with our independent determinations of the relationship between galaxy bias and stellar mass at these redshifts and appears to be an interesting method to investigate the coevolution of these quantities in the future. Finally, we investigate the SHMR. This indicates the efficiency with which baryons have been converted into stars over the lifetime of a dark matter halo. We fit the SHMR parametrization of Behroozi et al. ( 2013b ) for our two lowest redshift bins ( and ).