  The production of the neutron-capture isotopes beyond iron that we observe
today in the solar system is the result of the combined contribution of the
r-process, the s- process and possibly the i-process. Low-mass AGB (2 < M/Msun
< 3) and massive (M >10 Msun ) stars have been identified as the sites of the
s-process. In this work we consider the evolution and nucleosynthesis of
low-mass AGB stars. We provide an update of the NuGrid Set models, adopting the
same general physics assumptions but using an updated convective-boundary
mixing model accounting for the contribution from internal gravity waves. The
combined data set includes the initial masses Mzams/Msun = 2, 3 for Z = 0.03,
0.02, 0.01. These models are computed with the MESA stellar code and the
evolution is followed up to the end of the AGB phase. The nucleosynthesis was
calculated for all isotopes in post-processing with the NuGrid mppnp code. The
convective boundary mixing model leads to the formation of a 13C-pocket three
times wider compared to the one obtained in the previous set of models,
bringing the simulation results now in closer agreement with observations. We
also discuss the potential impact of other processes inducing mixing, like
rotation, adopting parametric models compatible with theory and observations.
Complete yield data tables, derived data products and online analytic data
access are provided.

Solar and Stellar Astrophysics