  We investigate the nucleosynthesis in the neutrino-driven winds blown off
from a $3M_\odot$ massive proto-neutron star (mPNS) temporarily formed during
the collapse of a $100M_\odot$ star. Such mPNSs would be formed in hypernovae.
We construct steady and spherically symmetric wind solutions. We set large
neutrino luminosities of $\sim 10^{53}\ {\rm erg\ s^{-1}}$ and average energies
of electron neutrinos and antineutrinos in the ranges of
$\epsilon_{\nu_e}=9-16\ {\rm MeV}$ and $\epsilon_{\bar{\nu}_e}=11-18\ {\rm
MeV}$ based on a recent numerical relativity simulation. The wind solutions
indicate much shorter temperature-decrease timescale than that of the winds
from ordinary PNSs and, depending on $\epsilon_\nu$, the winds can be both
neutron-rich and proton-rich. In the neutron-rich wind, the $r$-process occurs
and the abundance distribution of a fiducial wind model of the mPNS gives an
approximate agreement with the abundance pattern of metal-poor weak $r$ star
HD~122563, although the third-peak elements are produced only when the
$\bar{\nu}_e$ energy is much larger than the $\nu_e$ energy. In the proton-rich
wind, the strong $\nu p$-process occurs and $A>100$ nuclides are synthesized.
The synthesized nuclei can be neutron-rich in some cases because the large
neutrino luminosity of the mPNS supplies a sufficient amount of neutrons.
