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tokens: is a mid-stage merger consisting of two face-on galaxies which appear to overlap and have a projected separation of ∼84 (6.3 kpc). Prominent rings/arms in each galaxy contain the bulk of the visible star clusters (Figure 19 ). The maximum A V adopted for this galaxy is 1.0 mag of visual extinction (see Figure 20 ; Miralles-Caballero et al. 2012 ). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 15 and 16 , respectively. 2MASX J08370182-4954302 2MASX J08370182-4954302 is a mid-stage merger containing two nuclei separated by ∼066 (0.36 kpc). Surrounding the nuclei are multiple bright star clusters in a spiral ridge just northwest and west of the nuclei (Figure 21 ). The maximum A V adopted for this galaxy is 3.7 mag of visual extinction (see Figure 22 ; Rich et al. 2012 ). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 17 and 18 , respectively. NGC 2623 Evans et al. ( 2008 ) discuss the detailed morphology of this galaxy at length. NGC 2623 is a late-stage merger with dust lanes running along its tidal tails into the nucleus. Several bright clusters are distributed throughout the bulge and in a “pie-wedge” concentration south of the nucleus (Figure 23 ). The maximum A V adopted for this galaxy is 1.9 mag of visual extinction (see Figure 24 ; Privon et al. 2013 ). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 19 and 20 , respectively. UGC 04881 UGC 04881 is an early-stage merger containing two nuclei separated by ∼11′′ (9 kpc). Spiral dust lanes and strings of star clusters surround the NE nucleus. In the SW nucleus, a linear distribution of star clusters and a prominent dust lane are seen (Figure 25 ). The maximum A V adopted for this galaxy is 1.9 mag of visual extinction (see Figure 26 ; González-Martín et al. 2009 ). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 21 and 22 , respectively. IC 2545 IC 2545 is a late-stage merger being viewed face on. Dust lanes and strings of star clusters extend from two unresolved nuclei separated by ∼08 (0.54 kpc) in the center of the galaxy. Multiple star clusters are also visible throughout the tidal tails (Figure 27 ). The maximum A V adopted for this galaxy is 4.0 mag of visual extinction (see Figure 28 ; van den Broek et al. 1991 ). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 23 and 24 , respectively. NGC 3256 NGC 3256 is a late-stage merger containing a large number of star clusters along the inner (∼20′′, or 4 kpc) spiral structure of the nuclear region. The spiral dust lanes extending from the nucleus give this galaxy pockets of high and low extinction (Figure 29 ). The maximum A V adopted for this galaxy is 3.3 mag of visual extinction (see Figure 30 ; Rich et al. 2012 ). The observed and derived