  We present optical UBVRI photometry and low-to-medium resolution
spectroscopic observations of type Iax SN 2020sck spanning -5.5 d to +67 d from
maximum light in the B-band. From the photometric analysis we find $\Delta
m_{\rm{B}}$(15) = 2.03$\pm$0.05 mag and $M_{\rm{B}}$=-17.81$\pm$0.22 mag.
Radiation diffusion model fit to the quasi-bolometric light curve indicates
0.13$\pm$0.02 $M_{\odot}$ of $^{56}$Ni and 0.34 $M_{\rm \odot}$ of ejecta are
synthesized in the explosion. Comparing the observed quasi-bolometric light
curve with angle-averaged bolometric light curve of three-dimensional pure
deflagration explosion of $M_{\rm{ch}}$ carbon-oxygen white dwarf, we find
agreement with a model in which 0.16 $M_{\odot}$ of $^{56}$Ni and 0.37
$M_{\odot}$ of ejecta is formed. By comparing the +1.4 day 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 H$\alpha$ ($\lambda$6563) line is
0.09 $M_{\odot}$ yr$^{-1}$ indicating a relatively young stellar environment.
