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The Bayesian isochrone fitting using the Markov chain Monte Carlo algorithmis applied, to derive the probability distribution of the parameters age,metallicity, reddening, and absolute distance modulus. We introduce the\texttt{SIRIUS} code by means of simulated color-magnitude diagrams, includingthe analysis of multiple stellar populations. The population tagging is appliedfrom the red giant branch to the bottom of the main sequence. Through sanitychecks using synthetic {\it HST} color-magnitude diagrams of globular clusterswe verify the code reliability in the context of simple and multiple stellarpopulations. In such tests, the formal uncertainties in age or age difference,metallicity, reddening, and absolute distance modulus can reach $400$ Myr,$0.03$ dex, $0.01$ mag, and $0.03$ mag, respectively. We apply the method toanalyse NGC 6752, using Dartmouth stellar evolutionary models. Assuming asingle stellar population, we derive an age of $13.7\pm0.5$ Gyr and a distanceof $d_{\odot}=4.11\pm 0.08$ kpc, with the latter in agreement within $~3\sigma$with the inverse Gaia parallax. In the analysis of the multiple stellarpopulations, three {populations} are clearly identified. From the ChromosomeMap and UV/Optical two-color diagrams inspection, we found a fraction of starsof $25\pm5$, $46\pm7$, and $29\pm5$ per cent, for the first, second, and thirdgenerations, respectively. These fractions are in good agreement with theliterature. An age difference of $500\pm410$ Myr between the first and thethird generation is found, with the uncertainty decreasing to $400$ Myr whenthe helium enhancement is taken into account.

Self-consistent analysis of stellar clusters: An application to HST data of the halo globular cluster NGC 6752