  Magnetorotational supernovae are a rare type of core-collapse supernovae
where the magnetic field and rotation play a central role in the dynamics of
the explosion. We present the post-processed nucleosynthesis of
state-of-the-art neutrino-MHD supernova models that follow the post explosion
evolution for few seconds. We find three different dynamical mechanisms to
produce heavy r-process elements: i) a prompt ejection of matter right after
core bounce, ii) neutron-rich matter that is ejected at late times due to a
reconfiguration of the protoneutronstar shape, iii) small amount of mass
ejected with high entropies in the center of the jet. We investigate total
ejecta yields, including the ones of unstable nuclei such as $^{26}$Al,
$^{44}$Ti, $^{56}$Ni, and $^{60}$Fe. The obtained $^{56}$Ni masses vary between
$0.01 - 1\,\mathrm{M_\odot}$. The latter maximum is compatible with hypernova
observations. Furthermore, all of our models synthesize Zn masses in agreement
with observations of old metal-poor stars. We calculate simplified light curves
to investigate whether our models can be candidates for superluminous
supernovae. The peak luminosities obtained from taking into account only
nuclear heating reach up to a few $\sim 10^{43} \,\mathrm{erg\,s^{-1}}$. Under
certain conditions, we find a significant impact of the $^{66}$Ni decay chain
that can raise the peak luminosity up to $\sim 38\%$ compared to models
including only the $^{56}$Ni decay chain. This work reinforces the theoretical
evidence on the critical role of magnetorotational supernovae to understand the
occurrence of hypernovae, superluminous supernovae, and the synthesis of heavy
elements.
