  We provide a set of stellar evolution and nucleosynthesis calculations that
applies established physics assumptions simultaneously to low- and
intermediate-mass and massive star models. Our goal is to provide an internally
consistent and comprehensive nuclear production and yield data base for
applications in areas such as pre-solar grain studies. Our non-rotating models
assume convective boundary mixing where it has been adopted before. We include
8 (12) initial masses for $Z = 0.01$ ($0.02$). Models are followed either until
the end of the asymptotic giant branch phase or the end of Si burning,
complemented by a simple analytic core-collapse supernova models with two
options for fallback and shock velocities. The explosions show which
pre-supernova yields will most strongly be effected by the explosive
nucleosynthesis. We discuss how these two explosion parameters impacts the
light elements and the $s$ and $p$ process. For low- and intermediate-mass
models our stellar yields from H to Bi include the effect of convective
boundary mixing at the He-intershell boundaries and the stellar evolution
feedback of the mixing process that produces the $^{13}$C pocket. All
post-processing nucleosynthesis calculations use the same nuclear reaction rate
network and nuclear physics input. We provide a discussion of the nuclear
production across the entire mass range organized by element group. All our
stellar nucleosynthesis profile and time evolution output is available
electronically, and tools to explore the data on the NuGrid VOspace hosted by
the Canadian Astronomical Data Centre are introduced.
