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 \approx 1.95 hours and 0.0849767 d \approx 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 } | \sim 3 \times 10 ^ { -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 \approx 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 _ { \odot } .