  We present the results of 11 nights of CCD unfiltered photometry of V4743 Sgr
(Nova Sgr 2002 # 3) from 2003 and 2005. We find two periods of 0.2799 d ~ 6.7 h
and 0.01642 d ~ 24 min in the 2005 data. The long period is also present in the
2003 data, but only weak evidence of the shorter period is found in this year.
The 24-min period is somewhat longer than the 22-min period, which was detected
from X-ray observations. We suggest that the 6.7-h periodicity represents the
orbital period of the underlying binary system and that the 24-min period is
the beat periodicity between the orbital period and the X-ray period, which is
presumably the spin period of the white dwarf. Thus, V4743 Sgr should be
classified as an intermediate polar (DQ Her star). About six months after the
nova outburst, the optical light curve of V4743 Sgr seemed to show
quasi-periodic oscillations, which are typical of the transient phase in
classical nova. Therefore, our results support the previous suggestion that the
trans ition phase in novae may be related to intermediate polars.
