  An essential factor in determining the flow characteristics of an accretion
flow is its angular momentum. According to the angular momentum of the flow,
semi-analytical analysis suggests various types of accretion solutions. It is
critical to test it with numerical simulations using the most advanced
framework available (general relativistic magnetohydrodynamics) to understand
how flow changes with different angular momentum. By changing the initial
condition of the accretion torus minimally, we can simulate steady, low angular
momentum accretion flow around a Kerr black hole. We focus primarily on the
lower limits of angular momentum and come upon that accretion flow with an
intermediate range of angular momentum differs significantly from high or very
low angular momentum flow. The intermediate angular momentum accretion flow has
the highest density, pressure, and temperature near the black hole, making it
easier to observe. We find that the density and pressure have power-law
scalings $\rho\propto r^{n-3/2}$ and $p_g\propto r^{n-5/2}$ which only hold for
very low angular momentum cases. With the increase in flow angular momentum, it
develops a non-axisymmetric nature. In this case, simple self-similarity does
not hold. We also find that the sonic surface moves away from the innermost
stable circular orbit as its angular momentum decreases. Finally, we emphasize
that intermediate angular momentum flow could provide a possible solution to
explain the complex observation features of the supermassive black hole
Sgr~A$^*$ at our galactic center.
