  The study of pulsating stars in eclipsing binaries holds the promise of
combining two different ways of measuring the physical properties of a star to
obtain improved constraints on stellar theory. Gravity (g) mode pulsations such
as those found in $\gamma$ Doradus stars can be used to probe rotational
profiles, mixing and magnetic fields. Until recently few $\gamma$ Doradus stars
in eclipsing binaries were known. We have discovered g-mode pulsations in four
detached eclipsing binary systems from light curves obtained by the Transiting
Exoplanet Survey Satellite (TESS) and present an analysis of their eclipses and
pulsational characteristics. We find unresolved g-mode pulsations at
frequencies 1--1.5 d$^{-1}$ in CM Lac, and measure the masses and radii of the
component stars from the TESS data and published radial velocities. MZ Lac
shows a much richer frequency spectrum, including pressure modes and
tidally-excited g-modes. RX Dra is in the northern continuous viewing zone of
TESS so has a light curve covering a full year, but shows relatively few
pulsation frequencies. For V2077 Cyg we formally measure four pulsation
frequencies, but the available data are inadequate to properly resolve the
g-mode pulsations. V2077 Cyg also shows total eclipses, with which we obtain
the first measurement of the surface gravity of the faint secondary star. All
four systems are bright and good candidates for detailed study. Further TESS
observations are scheduled for all four systems, with much improved temporal
baselines in the cases of RX Dra and V2077 Cyg.
