  G31.41+0.31 is a well known chemically rich hot molecular core (HMC). Using
Band 3 observations of Atacama Large Millimeter Array (ALMA), we have analyzed
the chemical and physical properties of the source. We have identified methyl
isocyanate (CH3NCO), a precursor of prebiotic molecules, towards the source. In
addition to this, we have reported complex organic molecules (COMs) like
methanol (CH3OH), methanethiol (CH3SH), and methyl formate (CH3OCHO).
Additionally, we have used transitions from molecules like HCN, HCO+, SiO to
trace the presence of infall and outflow signatures around the star-forming
region. For the COMs, we have estimated the column densities and kinetic
temperatures, assuming molecular excitation under local thermodynamic
equilibrium (LTE) conditions. From the estimated kinetic temperatures of
certain COMs, we found that multiple temperature components may be present in
the HMC environment. Comparing the obtained molecular column densities between
the existing observational results toward other HMCs, it seems that the COMs
are favourably produced in the hot-core environment ($\sim 100$ K or higher).
Though the spectral emissions towards G31.41+0.31 are not fully resolved, we
find that CH$_3$NCO and other COMs are possibly formed on the grain/ice phase
and populate the gas environment similar to other hot cores like Sgr B2, Orion
KL, and G10.47+0.03, etc.
