  We present the comprehensive analysis of the high-amplitude $\delta$ Sct star
V2367 Cygni. Firstly, we perform the frequency analysis for the whole available
set of the {\it Kepler} and {\it TESS} photometry. Most of the frequency peaks
are harmonics or combinations of the three known independent frequencies with
the highest amplitudes, i.e., $\nu_1=5.66106$\,d$^{-1}$,
$\nu_2=7.14898$\,d$^{-1}$ and $\nu_3=7.77557$\,d$^{-1}$. The total number of
independent frequencies is 26 and 25 from the {\it Kepler} and {\it TESS} light
curve, respectively. Then, using the $UBVRI$ time-series photometry, we
unambiguously identify the dominant frequency $\nu_1$ as the radial mode,
whereas in the case of frequencies $\nu_2$ and $\nu_3$ the most probable mode
degrees are $\ell=0$ or $\ell=2$. However, only the frequency $\nu_2$ can be
associated with a radial mode, and only if higher order effects of rotation are
taken into account. Including the rotational mode coupling, we constructed
complex seismic models of V2367\,Cyg, which fit $\nu_1$ and $\nu_2$ as radial
modes, and reproduce the amplitude of bolometric flux variations (the parameter
$f$) for the dominant mode. The empirical values of $f$ are derived from the
$UBVRI$ amplitudes and phases. We rely on the Bayesian analysis based on Monte
Carlo simulations to derive constraints on evolutionary stage, mass, rotation,
overshooting from the convective core and efficiency of convective transport in
the envelope. Our seismic analysis clearly indicates that V2367\,Cyg is in a
post-MS phase of evolution. This is the first extensive seismic modelling that
takes into account the effect of rotational coupling between pulsation modes.
