  We have attempted to mitigate the challenge of connecting the neutron star
(NS) properties with the nuclear matter parameters that describe equations of
state (EoSs). The efforts to correlate various neutron star properties with
individual nuclear matter parameters have been inconclusive. A Principal
Component Analysis is employed as a tool to uncover the connection between
multiple nuclear matter parameters and the tidal deformability as well as the
radius of neutron stars within the mass range of $1.2-1.8M_\odot$. The
essential EOSs for neutron star matter at low densities have been derived using
both uncorrelated uniform distributions and minimally constrained joint
posterior distributions of nuclear matter parameters. For higher densities
($\rho > 0.32$fm$^{-3}$), the EOSs have been established through a suitable
parameterization of the speed of sound, which consistently maintains causality
and gradually approaches the conformal limit. Our analysis reveals that in
order to account for over 90\% of the variability in NS properties, it is
crucial to consider two or more principal components, emphasizing the
significance of employing multivariate analysis. To explain the variability in
tidal deformability needs a greater number of principal components compared to
those for the radius at a given NS mass. The contributions from iso-vector
nuclear matter parameters to the tidal deformability and radius of NS decrease
by $\sim$ 25\% with the increase in mass of NS from 1.2$M_\odot$ to
1.8$M_\odot$.
