We present high-speed , three-colour photometry of the eclipsing cataclysmic variable SDSS J170213.26+322954.1 ( hereafter SDSS J1702+3229 ) .
This system has an orbital period of 2.4 hours , placing it within the “ period gap ” for cataclysmic variables .
We determine the system parameters via a parameterized model of the eclipse fitted to the observed light curve by \chi ^ { 2 } minimization .
We obtain a mass ratio of q = 0.215 \pm 0.015 and an orbital inclination i = 82 ^ { \circ } .4 \pm 0 ^ { \circ } .4 .
The primary mass is M _ { \mathrm { w } } = 0.94 \pm 0.01 M _ { \sun } .
The secondary mass and radius are found to be M _ { \mathrm { r } } = 0.20 \pm 0.01 M _ { \sun } and R _ { \mathrm { r } } = 0.243 \pm 0.013 R _ { \sun } respectively .
We find a distance to the system of 440 \pm 30 pc , and an effective temperature for the secondary star of 3800 \pm 100 K ( corresponding to a spectral type of M0 \pm 0.5V ) .
Both the distance and effective temperature are consistent with previous values derived via spectroscopy of the red star .

The secondary star is significantly less massive than expected for the orbital period , and significantly warmer than expected for its mass .
This can be explained if the secondary star is significantly evolved : the mass and effective temperature are consistent with a secondary star that began mass transfer with a greatly reduced central hydrogen fraction .
The nature of the secondary star in SDSS J1702+3229 supports predictions that CVs with evolved secondary stars might be found accreting within the period gap .