  Low mass stars ($\leq 1$ M$_{\odot}$) are some of the best candidates for
hosting planets with detectable life because of these stars' long lifetimes and
relative planet to star mass and radius ratios. An important aspect of these
stars to consider is the amount of ultraviolet (UV) and X-ray radiation
incident on planets in the habitable zones due to the ability of UV and X-ray
radiation to alter the chemistry and evolution of planetary atmospheres. In
this work, we build on the results of the HAZMAT I (Shkolnik & Barman 2014) and
HAZMAT III (Schneider & Shkolnik 2018) M star studies to determine the
intrinsic UV and X-ray flux evolution with age for M stars using Gaia
parallactic distances. We then compare these results to the intrinsic fluxes of
K stars adapted from HAZMAT V (Richey-Yowell et al. 2019). We find that
although the intrinsic M star UV flux is 10 to 100 times lower than that of K
stars, the UV fluxes in their respective habitable zone are similar. However,
the habitable zone X-ray flux evolutions are slightly more distinguishable with
a factor of 3 -- 15 times larger X-ray flux for late-M stars than for K stars.
These results suggest that there may not be a K dwarf advantage compared to M
stars in the UV, but one may still exist in the X-ray.
