  The goal of this work is to probe the total mass distribution of early-type
galaxies with globular clusters (GCs) as kinematic tracers, by constraining the
parameters of the profile with a flexible modelling approach. To that end, we
leverage the extended spatial distribution of GCs from the SLUGGS survey
($\langle R_{\rm GC,\ max} \rangle \sim 8R_{\rm e}$) in combination with
discrete dynamical modelling. We use discrete Jeans anisotropic modelling in
cylindrical coordinates to determine the velocity moments at the location of
the GCs in our sample. We use a Bayesian framework to determine the best-fit
parameters of the total mass density profile and orbital properties of the GC
systems. We find that the orbital properties (anisotropy and rotation of the
dispersion-dominated GC systems) minimally impact the measurements of the inner
slope and enclosed mass, while a strong presence of dynamically-distinct
subpopulations or low numbers of kinematic tracers can bias the results. Owing
to the large spatial extent of the tracers our method is sensitive to the
intrinsic inner slope of the total mass profile and we find $\overline{\alpha}
= -1.88\pm 0.01$ for 12 galaxies with robust measurements. To compare our
results with literature values we fit a single power-law profile to the
resulting total mass density. In the radial range 0.1-4~$R_{\rm e}$ our
measured slope has a value of $\langle \gamma_{\rm tot}\rangle = -2.22\pm0.14$
and is in good agreement with the literature.
