Mass and energy flow of BH accretion and feedback. This study extends the framework of star formation in Grudić et al. (2018) and BH accretion without feedback in Paper I. To implement BH feedback, we use a model of mass transfer from the disk to the BH. With only a fraction of the accretion flow going to the BH, other portions are deposited back to the GMC in the form of radiation, jets and winds, and cosmic rays. We note that since the feedback energy efficiencies are typically small (≲0.1), ${\dot{M}}_{\mathrm{BH}}\doteq {\dot{M}}_{\mathrm{BH},0}$.