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tokens: Dynamical Time, J2000.0 ecliptic and equinox). Source: JPL’s SBDB (solution date, 2020-Mar-03 08:13:59). The orbit determination in Table 1 is still uncertain and its associated evolution rather chaotic (see Section 3 ). Wiegert, Innanen Mikkola ( 1998 ) have shown that the statistical analysis of an extensive set of numerical simulations accounting for the uncertainties associated with an orbit determination can produce reliable results. In order to obtain sufficiently robust conclusions, we apply the Monte Carlo using the Covariance Matrix (MCCM) method detailed in section 3 of de la Fuente Marcos de la Fuente Marcos ( 2015b ) to generate initial conditions for our N -body simulations that have been carried out using Aarseth’s implementation of the Hermite integrator (Aarseth 2003 ); the direct N -body code is publicly available. 1 The covariance matrix required to generate initial positions and velocities for 10 4 control or clone orbits has been obtained from Jet Propulsion Laboratory’s Solar System Dynamics Group Small-Body Database (JPL’s SSDG SBDB, Giorgini 2015 ). 2 This is also the source of the data in Table 1 ; JPL’s horizons 3 ephemeris system (Giorgini Yeomans 1999 ) has been used to gather most input data used in our calculations (e.g. data in Table 2 ). Some data have been retrieved from JPL’s SBDB using the tools provided by the Python package Astroquery (Ginsburg et al. 2019 ; Mommert et al. 2019 ). Extensive details on our calculations and physical model can be found in de la Fuente Marcos de la Fuente Marcos ( 2012 ), de la Fuente Marcos de la Fuente Marcos ( 2018a ), and de la Fuente Marcos de la Fuente Marcos ( 2018b ). Table 2. Cartesian state vector of 2020 CD 3 : components and associated 1σ uncertainties. Epoch as in Table 1 . Source: JPL’s SBDB. In order to analyse the results, we produced histograms using the Matplotlib library (Hunter 2007 ) with sets of bins of constant size computed using Astropy (Astropy Collaboration 2013 , 2018 ) by applying the Freedman and Diaconis rule (Freedman Diaconis 1981 ). Instead of using frequency-based histograms, we considered counts to form a probability density so that the area under the histogram will sum to one. 3 ORBITAL EVOLUTION With our calculations, we aimed at answering four main questions: (i) When did this capture take place? (ii) When is 2020 CD 3 leaving its current geocentric path? (iii) How was the pre-capture orbit of 2020 CD 3 ? (iv) How diverse is the evolution in the neighbourhood of the initial conditions in Table 2 ? Answering the first two questions, we can find out if 2020 CD 3 is experiencing a temporarily captured fly-by or a temporarily captured orbiter episode. The third question is directly related to the origin of 2020 CD 3 and the fourth question can inform us on the reliability of our results. In order to provide robust answers to all these questions, we first focus on the initial conditions in the form of Cartesian state vectors and then we use