  In this paper we analyzed the light curve of the object KIC~3832716 observed
during Kepler K1 mission. We showed that this previously known eclipsing binary
is in fact quadruple system, in double eclipsing binary configuration on a long
period orbit with the mass ratio of eclipsing binaries $0.7 \pm 0.3$. The
system consists of eclipsing binary A with the orbital period of $P_A \sim
1.1419$\,d. Eclipsing binary A contains larger but less luminous secondary
component in the post main sequence stage of its evolution consistent with an
"Algol paradox" which can explain parameters of the components by mass transfer
from secondary component after leaving the main sequence. Inspection of the
light curve and eclipse time variations of the eclipsing binary A also
indicates the presence of spots on the surface of secondary component with
$57$\,d period of activity probably induced by longitudonal motion of the
spots. The second eclipsing binary B with orbital period $P_B \sim 2.1703$\,d
contains very dim secondary component with luminosity below 0.09\,$L_{\odot}$.
