  Recently there has been an interest in exploring black holes that are regular
in the sense that the central curvature singularity is avoided. Here, we depict
a method to obtain a regular black hole (RBH) spacetime $(\mathcal{M},
\Tilde{g})$ from the unhindered gravitational collapse from regular initial
data of a spherically symmetric perfect fluid $(\mathcal{M}, g)$. In other
words, we obtain the equilibrium metric $\Tilde g$ as a limiting case of the
time-evolving metric $g$. In the spirit of Joshi, Malafarina and Narayan
(\textit{Class. Quantum Grav. 31, 015002, 2014}), our description of
gravitational collapse is implicit in nature in the sense that we do not
describe the data at each time-slice. Rather, we impose a condition in terms of
geometric and matter variables for the collapse to have an end-state that is
devoid of incomplete geodesics but admits a marginally trapped surface (MTS).
The admission of MTS causally disconnects two mutually exclusive regions
$\Hat{\mathcal{M}}_1$ and $\Hat{\mathcal{M}}_2\subset \mathcal{M}$ in the sense
that $\forall~p\in\Hat{\mathcal{M}_2}$, the causal past of $p$ does not
intersect $\Hat{\mathcal{M}}_1$. While the classic Oppenheimer-Snyder collapse
model necessarily produces a black hole with a Schwarzschild singularity at the
centre, we show here that there are classes of regular initial conditions for
which the collapse gives rise to a RBH.
