  We determine the age of the eclipsing binary V380 Cygni, whose components
have a significant mass ratio, $M_B/M_A\approx$ 0.6. Because this binary
exhibits spectral lines of both components, the values of masses and radii
could be determined with a very high accuracy. Assuming that both components
are on the main sequence, we derive the age of about 16 Myr. However, in this
case the primary needs a large overshooting from the convective core
($f_{\rm{ov}} \approx 0.04$) and higher metallicity ($Z \approx 0.02$). It is
difficult to tell whether such a high value of overshooting from the convective
core is reliable or rather mimics other mixing processes, which took place on
the whole main sequence evolution, e.g., resulting from diffusion, rotation
etc. If the primary is already in the overall contraction phase or just after,
then the age of the system is about 13 Myr. Based on the available
observations, we cannot resolve what is the evolutionary stage of the V380 Cyg
system.
  The analysis of the Kepler light curve does not show any significant
periodicity besides the orbital frequency and, most probably, the rotational
frequency and their multiplets.
