  We present results of 32 nights of CCD photometry of V1974 Cygni, from the
years 1994 and 1995. We verify the presence of two distinct periodicities in
the light curve: 0.0812585 day~1.95 hours and 0.0849767 d~2.04 hr. We establish
that the shorter periodicity is the orbital period of the underlying binary
system. The longer period oscillates with an average value of |dot(P)| ~
3x10^(7)--typical to permanent superhumps. The two periods obey the linear
relation between the orbital and superhump periods that holds among members of
the SU Ursae Majoris class of dwarf novae. A third periodicity of 0.083204
d~2.00 hr appeared in 1994 but not in 1995. It may be related to the recently
discovered anti-superhump phenomenon. These results suggest a linkage between
the classical nova V1974 Cyg and the SU UMa stars, and indicate the existence
of an accretion disk and permanent superhumps in the system no later than 30
months after the nova outburst. From the precessing disk model of the superhump
phenomenon we estimate that the mass ratio in the binary system is between 2.2
and 3.6. Combined with previous results this implies a white dwarf mass of
0.75-1.07 M sun.
