  We observed the 2014 superoutburst of the SU UMa-type intermediate polar CC
Scl. We detected superhumps with a mean period of 0.05998(2) d during the
superoutburst plateau and during three nights after the fading. During the
post-superoutburst stage after three nights, a stable superhump period of
0.059523(6) d was detected. We found that this object is an eclipsing system
with an orbital period of 0.058567233(8) d. By assuming that the disk radius in
the post-superoutburst phase is similar to those in other SU UMa-type dwarf
novae, we obtained a mass ratio of q=0.072(3) from the dynamical precession
rate of the accretion disk. The eclipse profile during outbursts can be modeled
by an inclination of 80.6+/-0.5 deg. The 2014 superoutburst was preceded by a
precursor outburst and the overall appearance of the outburst was similar to
superoutbursts in ordinary SU UMa-type dwarf novae. We showed that the standard
thermal-tidal instability model can explain the outburst behavior in this
system and suggest that inner truncation of the disk by magnetism of the white
dwarf does not strongly affect the behavior in the outer part of the disk.
