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Massive stars are key sources of radiative, kinetic, and chemical feedback inthe universe. Grids of massive star models computed by different groups eachusing their own codes, input physics choices and numerical approximations,however, lead to inconsistent results for the same stars. We use three of these1D codes---GENEC, KEPLER and MESA---to compute non-rotating stellar models of$15~\mathrm{M}_\odot$, $20~\mathrm{M}_\odot$, and $25~\mathrm{M}_\odot$ andcompare their nucleosynthesis. We follow the evolution from the main sequenceuntil the end of core helium burning. The GENEC and KEPLER models hold physicsassumptions used in large grids of published models. The MESA code was set upto use convective core overshooting such that the CO core masses are consistentwith those obtained by GENEC. For all models, full nucleosynthesis is computedusing the NuGrid post-processing tool MPPNP.  We find that the surface abundances predicted by the models are in reasonableagreement. In the helium core, the standard deviation of the elementaloverproduction factors for Fe to Mo is less than $30\,\%$---smaller than theimpact of the present nuclear physics uncertainties. For our three initialmasses, the three stellar evolution codes yield consistent results. Differencesin key properties of the models, e.g., helium and CO core masses and the timespent as a red supergiant, are traced back to the treatment of convection and,to a lesser extent, mass loss. The mixing processes in stars remain the keyuncertainty in stellar modelling. Better constrained prescriptions are thusnecessary to improve the predictive power of stellar evolution models.

Code dependencies of pre-supernova evolution and nucleosynthesis in massive stars: Evolution to the end of core helium burning