  In a previously presented proof-of-principle study, we established a
parametrized spherically symmetric explosion method (PUSH) that can reproduce
many features of core-collapse supernovae for a wide range of pre-explosion
models. The method is based on the neutrino-driven mechanism and follows
collapse, bounce and explosion. There are two crucial aspects of our model for
nucleosynthesis predictions. First, the mass cut and explosion energy emerge
simultaneously from the simulation (determining, for each stellar model, the
amount of Fe-group ejecta). Second, the interactions between neutrinos and
matter are included consistently (setting the electron fraction of the
innermost ejecta). In the present paper, we use the successful explosion models
from Ebinger et al. (2018) which include two sets of pre-explosion models at
solar metallicity, with combined masses between 10.8 and 120 M$_{\odot}$. We
perform systematic nucleosynthesis studies and predict detailed isotopic
yields. The resulting $^{56}$Ni ejecta are in overall agreement with
observationally derived values from normal core-collapse supernovae. The
Fe-group yields are also in agreement with derived abundances for metal-poor
star HD84937. We also present a comparison of our results with observational
trends in alpha element to iron ratios.
