  We investigate the structure of relativistic, low-angular momentum, inviscid
advective accretion flow in a stationary axisymmetric Kerr-like wormhole (WH)
spacetime, characterized by the spin parameter ($a_{\rm k}$), the dimensionless
parameter ($\beta$), and the source mass ($M_{\rm WH}$). In doing so, we
self-consistently solve the set of governing equations describing the
relativistic accretion flow around a Kerr-like WH in the steady state, and for
the first time, we obtain all possible classes of global accretion solutions
for transonic as well as subsonic flows. We study the properties of dynamical
and thermodynamical flow variables and examine how the nature of the accretion
solutions alters due to the change of the model parameters, namely energy
($\mathcal{E}$), angular momentum ($\lambda$), $a_{\rm k}$, and $\beta$.
Further, we separate the parameter space in $\lambda-\mathcal{E}$ plane
according to the nature of the flow solutions, and study the modification of
the parameter space by varying $a_{\rm k}$ and $\beta$. Moreover, we retrace
the parameter space in $a_{\rm k}-\beta$ plane that allows accretion solutions
containing multiple critical points. Finally, we calculate the disc luminosity
($L$) considering free-free emissions for transonic solutions as these
solutions are astrophysically relevant and discuss the implication of this
model formalism in the context of astrophysical applications.
