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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 Δm_B(15) = 2.03 ± 0.05 mag and M_B = -17.81 ± 0.22 mag. Radiation diffusion model fit to the quasi-bolometric light curve indicates 0.13 ± 0.02 M_☉ of ⁵⁶Ni and 0.34 M_☉ 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 M_ch carbon-oxygen white dwarf, we find agreement with a model in which 0.16 M_☉ of ⁵⁶Ni and 0.37 M_☉ 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 C II, C III, and O I. 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 Hα (λ6563) line is 0.09 M_☉ yr^–1, indicating a relatively young stellar environment.