Stellar mass–halo mass relation (top) and black hole mass–stellar mass relation (bottom) for the light-seeding (left), fiducial-seeding (center), and early-seeding (right) models. The shaded region, which represents the empirical relation at z = 1 (P. S. Behroozi et al. 2010), should be treated as a guide for the eye, as we overplot results from all redshifts. For seed black holes with M_BH < 10⁷M_⊙, the black hole does not grow, and the galaxy is not quenched, regardless of feedback efficiencies, resulting in excess stellar mass above M_Halo ≳ 10¹²M_⊙. In the fiducial seeding case, the black hole overgrows without feedback, grows moderately when the efficiency matches a_* = 0 result, and fails to accrete when the efficiency corresponds to maximum spin (η ≳ 0.3); star formation is also quenched in this high-efficiency case. With early massive seeding, black holes still do not grow through accretion for η ≳ 0.3, but growth through mergers can reproduce the observed local black hole–stellar mass relation. Galaxy quenching is also more efficient, yielding better agreement with the local stellar mass–halo mass relation.