  We analyze K2 light curves for 132 low-mass ($1\ \gtrsim\ M_*\ \gtrsim\
0.1$~${M_{\odot}}$) members of the 600--800~Myr-old Hyades cluster and measure
rotation periods ($P_{rot}$) for 116 of these stars. These include 93 stars
with no prior $P_{rot}$ measurement; the total number of Hyads with known
$P_{rot}$ is now 232. We then combine literature binary data with Gaia DR2
photometry and astrometry to select single star sequences in the Hyades and its
roughly coeval Praesepe open cluster, and derive a new reddening value of $A_V
= 0.035$$\pm$$0.011$ for Praesepe. Comparing the effective
temperature--$P_{rot}$ distributions for the Hyades and Praesepe, we find that
solar-type Hyads rotate, on average, 0.4~d slower than their Praesepe
counterparts. This $P_{rot}$ difference indicates that the Hyades is slightly
older than Praesepe: we apply a new gyrochronology model tuned with Praesepe
and the Sun, and find an age difference between the two clusters of 57~Myr.
However, this $P_{rot}$ difference decreases and eventually disappears for
lower-mass stars. This provides further evidence for stalling in the rotational
evolution of these stars, and highlights the need for more detailed analysis of
angular-momentum evolution for stars of different masses and ages.
