Notes. The SN IIP, SN 1987A-like and SN IIn categories only include our accretor models, and the reported ranges only differ in a few quantities when neglecting models that likely experience enhanced LBV-like mass loss (modified ranges shown in parentheses). Provided are the central specific entropy s_c of stars at core collapse, the compactness ξ_2.5, the CO core masses M_CO, the final stellar masses M_cc, the SN ejecta masses M_ej, the mass of the hydrogen-rich envelope M_H, env of the SN progenitors, the radii R_cc, the effective temperature T_eff, cc and luminosity log L_cc/L_⊙ of the pre-SN models, the explosion energy E_expl, nickel mass M_Ni, NS kick velocity v_kick, logarithmic E_expl to M_ej ratio (in units of erg g⁻¹) and the average ejecta velocity $v_{\mathrm{sn}}=\sqrt{2E_{\mathrm{expl}}/M_{\mathrm{ej}}}$. All numbers are rounded to the last shown digit except for R_cc, v_kick and v_sn, which are rounded to the nearest 50 R_⊙, 50 km s⁻¹ and 100 km s⁻¹, respectively. The value ranges in parentheses exclude stars that likely experience significant LBV-like mass loss, i.e. spend more than 10⁴ yr as LBVs. For CO core masses around ≈7 M_⊙, there are no SN explosions because these models are predicted to directly collapse into BHs (c.f. Paper I). For individual numbers and further quantities, see Table A.1.