  We report long baseline interferometric observations with the CHARA Array
that resolve six previously known double-lined spectroscopic binary systems in
the Hyades cluster, with orbital periods ranging from 3 to 358 days: HD 27483,
HD 283882, HD 26874, HD 27149, HD 30676, and HD 28545. We combine those
observations with new and existing radial-velocity measurements, to infer the
dynamical masses for the components as well as the orbital parallaxes. For most
stars the masses are determined to better than 1%. Our work significantly
increases the number of systems with mass determinations in the cluster. We
find that while current models of stellar evolution for the age and metallicity
of the Hyades are able to reproduce the overall shape of the empirical
mass-luminosity relation, they overestimate the $V$-band fluxes by about 0.1
mag between 0.5 and 1.4 $M_{\odot}$. The disagreement is smaller in $H$, and
near zero in $K$, and depends somewhat on the model. We also make use of the
TESS light curves to estimate rotation periods for our targets, and detect
numerous flares in one of them (HD 283882), estimating an average flaring rate
of 0.44 events per day.
