  We present a detailed mass reconstruction of the cluster RCS0224-0002 at
$z=0.773$ from the strong lensing features observed with HST/WFPC2. The mass
profile is reconstructed using a parametric approach. We introduce a novel
method to fit extended multiple images based on the Modified Hausdorff Distance
between observed arcs and the arcs reproduced by the model. We perform the
detailed error analysis of the model parameter using the MCMC method. Our model
reproduces all the observed strong lensing features of the RCS0224-0002 and
predicts the redshift of one of the arcs systems to be $z\approx 2.65$ (the
other system has an spectroscopic redshift of $z=4.87$). The reconstructed
inner mass profile is well fitted by a non-singular isothermal sphere, rather
than with an NFW model. Dark matter substructure, derived from the light
distribution of the most luminous cluster members, is crucial for reproducing
the complexity of the quadrupole image system, which could not be achieved
otherwise. The reconstructed mass distribution closely follows the light,
however it is significantly shifted from the X-ray emission of the gas. The
mass of RCS0224-0002 derived from the lensing model, $\approx 2\times10^{14}
M_\odot$ is in a very good agreement with the one obtained from the X-ray
temperature measured with deep Chandra observations.
