We present optical UBVRI photometry and low-to-medium resolution spectroscopic observations of type Iax supernova SN 2020sck spanning -5.5 days to +67 days from maximum light in the B-band. From the photometric analysis we find {Delta}m_B_(15)=2.03+/-0.05mag and M_B_=-17.81+/-0.22mag. Radiation diffusion model fit to the quasi-bolometric light curve indicates 0.13+/-0.02M_{sun} of ^56^Ni and 0.34M{sun} of ejecta are synthesized in the explosion. Comparing the observed quasi-bolometric light curve with the angle-averaged bolometric light curve of a three-dimensional pure deflagration explosion of Mch carbon-oxygen white dwarf, we find agreement with a model in which 0.16M{sun} of ^56^Ni and 0.37M{sun} of ejecta is formed. By comparing the +1.4 days spectrum of SN 2020sck with synthetic spectrum generated using SYN++, we find absorption features due to CII, CIII, and OI. These are unburned materials in the explosion and indicate a C-O white dwarf. One- dimensional radiative transfer modeling of the spectra with TARDIS shows higher density in the ejecta near the photosphere and a steep decrease in the outer layers with an ejecta composition dominated mostly by C, O, Si, Fe, and Ni. The star-formation rate of the host galaxy computed from the luminosity of the H{alpha} ({lambda}6563) line is 0.09M{sun}_/yr, indicating a relatively young stellar environment.