We present the results of photometric analysis of WZ Sge type dwarf nova TCP J20171288+1156589. This object exhibited an outburst with a large amplitude of $>7.9$ magnitudes and was observed for over a month. The photometric evolution of the superoutburst was atypical for WZ Sge-type dwarf novae. Periodogram analysis reveals early superhumps with the most probable period of $0.0611\pm 0.0001$ days during the initial decline. After a plateau phase of approximately 11 days, ordinary superhumps (likely stage B) emerged with a period of $0.0616\pm 0.0001$ days, corresponding to a superhump excess of $\epsilon =0.008$ correspondingly. This delay in the onset of ordinary superhumps is an unusual feature among WZ Sge stars. We evaluated the main parameters of the system: mass ratio $q=M_{RD}/M_{WD}=0.06\pm 0.005$ , yielding component masses of $M_{WD}\sim 1.0\pm 0.15M_{\odot }$ for the white dwarf and $M_{RD}=0.06\pm 0.01M_{\odot }$ for the donor. The estimated distance to the system is $\sim 850$ pc, and the binary separation is $a=0.67\pm 0.03R_{\odot }$ .
