Notes. The first column lists the total mass of the stellar component, which originates in a gaseous cluster with total masses of 3 · 10⁶, 10⁶, 3 · 10⁵ M_⊙, respectively, given our adopted star formation efficiency, ε = 0.35. Subsequent columns list the stellar component Plummer radius, the initial compactness of the gaseous cluster before gas depletion, the depletion timescale, the maximum BH mass, the maximum BH spin, and the fit parameters of the median spin Eq. (31). The last column lists the median saturating spin with its 1σ percentile for m_BH ≥ 100 M_⊙. We chose compactness values that give similar τ ≲ τ_stall (Eq. (2)) for all cases, while covering the two primary cases of BH masses: either the maximum possible BH mass, $m_{\mathrm{B}\mathrm{H}}^{max}\approx {10}^3{\mathrm{M}}_{\odot }$, is generated, or the upper BH mass gap is marginally populated, $m_{\mathrm{B}\mathrm{H}}^{max}\approx 150{\mathrm{M}}_{\odot }$. Blue entries indicate a stellar cluster mass and size consistent with JWST observations of the Cosmic Gems clusters.