  We present the physical properties of EPIC 245932119 ($K_{\rm p}$ = $+$9.82)
exhibiting both eclipses and pulsations from the {\it K{\rm 2}} photometry. The
binary modeling indicates that the eclipsing system is in detached or
semi-detached configurations with a mass ratio of 0.283 or 0.245, respectively,
and that its light-curve parameters are almost unaffected by pulsations.
Multiple frequency analyses were performed for the light residuals in the
outside-primary eclipsing phase after subtracting the binarity effects from the
observed data. We detected 35 frequencies with signal to noise amplitude ratios
larger than 4.0 in two regions of 0.62$-$6.28 day$^{-1}$ and 19.36$-$24.07
day$^{-1}$. Among these, it is possible that some high signals close to the
Nyquist limit $f_{\rm Ny}$ may be reflections of real pulsation frequencies
(2$f_{\rm Ny}-f_i$). All frequencies ($f_8$, $f_9$, $f_{14}$, $f_{18}$,
$f_{24}$, $f_{32}$) in the lower frequency region are orbital harmonics, and
three high frequencies ($f_{19}$, $f_{20}$, $f_{22}$) appear to be sidelobes
split from the main frequency of $f_1$ = 22.77503 day$^{-1}$. Most of them are
thought to be alias effects caused by the orbital frequency. For the 26 other
frequencies, the pulsation periods and pulsation constants are in the ranges of
0.041$-$0.052 days and 0.013$-$0.016 days, respectively. These values and the
position in the Hertzsprung-Russell diagram reveal that the primary component
is a $\delta$ Sct pulsator. The observational properties of EPIC 245932119 are
in good agreement with those for eclipsing binaries with $\delta$ Sct-type
pulsating components.
