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We construct a model for the Galactic globular cluster system based on arealistic gravitational potential and a distribution function (DF) analytic inthe action integrals. The DF comprises disc and halo components whosefunctional forms resemble those recently used to describe the stellar discs andstellar halo. We determine the posterior distribution of our model parametersusing a Bayesian approach. This gives us an understanding of how well theglobular cluster data constrain our model. The favoured parameter values of thedisc and halo DFs are similar to values previously obtained from fits to thestellar disc and halo, although the cluster halo system shows clearer rotationthan does the stellar halo. Our model reproduces the generic features of theglobular cluster system, namely the density profile, the mean rotationvelocity. The fraction of disc clusters coincides with the observed fraction ofmetal-rich clusters. However, the data indicate either incompatibility betweencatalogued cluster distances and current estimates of distance to the GalacticCentre, or failure to identify clusters behind the bulge. As the data for ourGalaxy's components increase in volume and precision over the next few years,it will be rewarding to revisit the present analysis.

Modelling the Milky Way's globular cluster system