Notes. Columns 3–6 give the fraction, F_BH, m, of the cluster’s initial stellar mass that is converted into BHs; the fraction, f_{ret, BH, m}, of those retained in the cluster owing to sufficiently low natal kicks; the fraction, F_BH, n, of the cluster’s initial number of stars that is converted into BHs; and the fraction, f_{ret, BH, n}, of those retained in the cluster, respectively. In this table, f_{ret, BH, m} and f_{ret, BH, n} correspond to the standard, fallback-controlled natal kicks (Sect. 3.1) – Sect. 3.2 discusses how the retentions are affected by alternative natal-kick prescriptions, namely, the convection-asymmetry-driven kick results in nearly the same retention fractions, the collapse-asymmetry-driven kick leads to all retention fractions ≈1.0 and the neutrino-driven kick leads to all retention fractions ≈0.0. Such BH retention fractions are representative of those in a typical young massive or an open cluster or a low-mass GC in the Milky Way or a local-group galaxy.