  We present a search for an excess of neutrino interactions due to dark matter
in the form of Weakly Interacting Massive Particles (WIMPs) annihilating in the
galactic center or halo based on the data set of Super-Kamiokande-I, -II, -III
and -IV taken from 1996 to 2016. We model the neutrino flux, energy, and flavor
distributions assuming WIMP self-annihilation is dominant to $\nu
\overline{\nu}$, $\mu^+\mu^-$, $b\overline{b}$, or $W^+W^-$. The excess is in
comparison to atmospheric neutrino interactions which are modeled in detail and
fit to data. Limits on the self-annihilation cross section $\langle \sigma_{A}
V \rangle$ are derived for WIMP masses in the range 1 GeV to 10 TeV, reaching
as low as $9.6 \times10^{-23}$ cm$^3$ s$^{-1}$ for 5 GeV WIMPs in $b\bar b$
mode and $1.2 \times10^{-24}$ cm$^3$ s$^{-1}$ for 1 GeV WIMPs in $\nu \bar \nu$
mode. The obtained sensitivity of the Super-Kamiokande detector to WIMP masses
below several tens of GeV is the best among similar indirect searches to date.
