  Core-collapse supernova (CCSN) explosions powered by rotation and magnetic
fields present an interesting astrophysical site for nucleosynthesis that
potentially contributes to the production of $r$-process elements. Here we
present yields of the innermost ejecta in 3D magnetorotational CCSN models
simulated using the CoCoNuT-FMT code. Strong magnetic fields tap the rotational
energy of the proto-neutron star and lead to earlier and more energetic ($\sim
3\times 10^{51}$ erg) explosions than typical neutrino-driven CCSNe. Compared
to a reference non-magnetic model, the ejecta in the magnetorotational models
have much more neutron-rich components with Ye down to $\sim$0.25. Our
post-processing calculations with the reaction network SkyNet show significant
production of weak $r$-process elements up to mass number $\sim$130. We find
negligible differences in the synthesis of heavy elements between two
magnetorotational models with different initial field strength of 10$^{10}$ and
10$^{12}$ G, in accord with their similar explosion dynamics. The
magnetorotational models produce about $\sim$0.19 and 0.14 Msun of radioactive
$^{56}$Ni, on the low end of inferred hypernova nickel masses. The yields are
publicly available at Zenodo: doi:10.5281/zenodo.10578981 for comparison with
stellar abundance patterns, inclusion in modelling galactic chemical evolution,
and comparison with other yield calculations. Our results add to the yet
restricted corpus of nucleosynthesis yields from 3D magnetorotational supernova
simulations and will help quantify yield uncertainties.
