  V1363 Cyg is a cataclysmic variable (CV) and a post-nova. Our analysis of its
long-term optical activity used the archival data from the AAVSO database and
literature. We showed that the accretion disk of V1363 Cyg is exposed to the
thermal-viscous instability (TVI) for at least part of the time. The time
fraction spent in the high state or the outbursts dramatically changed on the
timescale of decades. Highly variable brightness of V1363 Cyg displayed several
episodes of a strong brightening (bumps in the light curve) from a cool disk in
the TVI zone. In the interpretation, their vastly discrepant decay rates show
that only some of these bumps can be attributed to the dwarf nova outbursts
without strong irradiation of the disk by the hot white dwarf. The Bailey
relation of the decay rate, if ascribed to a DN outburst of V1363 Cyg, speaks
in favor of its orbital period $P_{\rm orb}$ very long for a CV, about 20-40
hr. A dominant cycle length of about 435 d was present in the brightness
changes all the time, even when the disk was well inside the TVI zone. We
interpret it as modulation of the companion's mass outflow by differential
rotation of the active region(s).
