Left: comparison between the retained mass distribution of the BHs (inside a M_cl(0) ≈ 5 × 10⁴ M_⊙, r_h(0) ≈ 2 pc, initially single-only stars model cluster; see also Fig. 8) for the various natal-kick prescriptions considered in this work (legends; see Sects. 3.1 and 3.2). The F12-rapid+B16-PPSN/PSN remnant-mass model (Sect. 2.2) and Z = 0.0001 is assumed. The dashed histogram represents the natal mass distribution of the BHs for these remnant-mass model and Z. No BHs are retained in such clusters in the neutrino-driven-kick case (Sect. 3.2.3; Fig. 9). In contrast, nearly all BHs are retained if the kicks are collapse asymmetry driven. Right: natal mass distribution of NSs for the F12-rapid(+B16-PPSN/PSN) remnant-mass model (black histogram). The retained mass distributions of the NSs for the collapse-asymmetry-driven kick model at t ≈ 20 Myr and 60 Myr are also shown (grey and blue histograms, respectively). The marginally escaping NSs at 20 Myr (Sect. 3.2.4; Fig. 9, bottom panel) are all depleted by 60 Myr when only the low-/zero-kicked ECS-NSs retain in the cluster.