  We present spectroscopic and photometric analysis of the eclipsing binary
KIC\,7385478. We find that the system is formed by F1V + K4III-IV components.
Combining results from analysis of spectroscopic data and $Kepler$ photometry,
we calculate masses and radii of the primary and the secondary components as
M$_{1}$ = 1.71 $\pm$ 0.08 \Msun, M$_{2}$ = 0.37 $\pm$ 0.04 \Msun~ and R$_{1}$ =
1.59 $\pm$ 0.03\Rsun, R$_{2}$ = 1.90 $\pm$ 0.03\Rsun, respectively. Position of
the primary component in HR diagram is in the region of $\gamma$ Doradus type
pulsators and residuals from light curve modeling exhibit additional light
variation with a dominant period of $\sim$0.5 day. These are clear evidences of
the $\gamma$ Doradus type pulsations on the primary component. We also observe
occasional increase in amplitude of the residuals, where the orbital period
becomes the most dominant period. These may be attributed to the cool star
activity originating from the secondary component.
