  We report the discovery of the third tidally tilted pulsator, TIC 63328020.
Observations with the TESS satellite reveal binary eclipses with an orbital
period of 1.1057 d, and $\delta$ Scuti-type pulsations with a mode frequency of
21.09533 d$^{-1}$. This pulsation exhibits a septuplet of orbital sidelobes as
well as a harmonic quintuplet. Using the oblique pulsator model, the primary
oscillation is identified as a sectoral dipole mode with $l = 1, |m| = 1$. We
find the pulsating star to have $M_1 \simeq 2.5\, {\rm M}_\odot$, $R_1 \simeq 3
\, {\rm R}_\odot$, and $T_{\rm eff,1} \simeq 8000$ K, while the secondary has
$M_2 \simeq 1.1 \, {\rm M}_\odot$, $R_2 \simeq 2 \, {\rm R}_\odot$, and $T_{\rm
eff,2} \simeq 5600$ K. Both stars appear to be close to filling their
respective Roche lobes. The properties of this binary as well as the tidally
tilted pulsations differ from the previous two tidally tilted pulsators,
HD74423 and CO Cam, in important ways. We also study the prior history of this
system with binary evolution models and conclude that extensive mass transfer
has occurred from the current secondary to the primary.
