  We examine the effect of thermal conduction on the low-angular momentum hot
accretion flow (HAF) around non-rotating black holes accreting mass at very low
rate. While doing so, we adopt the conductive heat flux in the saturated form,
and solve the set of dynamical equations corresponding to a steady,
axisymmetric, viscous, advective accretion flow using numerical methods. We
study the dynamical and thermodynamical properties of accreting matter in terms
of the input parameters, namely energy ($\varepsilon_0$), angular momentum
($\ell_0$), viscosity parameter ($\alpha$), and saturation constant ($\Phi_{\rm
s}$) regulating the effect of thermal conduction. We find that $\Phi_{\rm s}$
plays a pivotal role in deciding the transonic properties of the global
accretion solutions. In general, when $\Phi_{\rm s}$ is increased, the critical
point ($r_{\rm c}$) is receded away from the black hole, and flow variables are
altered particularly in the outer part of the disc. To quantify the physically
acceptable range of $\Phi_{\rm s}$, we compare the global transonic solutions
with the self-similar solutions, and observe that the maximum saturation
constant ($\Phi^{\rm max}_{\rm s}$) estimated from the global solutions exceeds
the saturated thermal conduction limit ($\Phi_{\rm sc}$) derived from the
self-similar formalism. Moreover, we calculate the correlation between $\alpha$
and $\Phi^{\rm max}_{\rm s}$ and find ample disagreement between global
solutions and self-similar solutions. Further, using the global flow variables,
we compute the Bernoulli parameter ($Be$) which remains positive all throughout
the disc, although flow becomes loosely unbound for higher $\Phi_{\rm s}$.
Finally, we indicate the relevance of this work in the astrophysical context in
explaining the possibility of massloss/outflows from the unbound disc.
