  In this paper, we present the properties of 10 halo globular clusters with
luminosities $L\simeq 5-7\times 10^5{L_\odot}$ in the Local Group galaxy M33
using the images of {\it Hubble Space Telescope} Wide Field Planetary Camera 2
in the F555W and F814W bands. We obtained ellipticities, position angles and
surface brightness profiles for them. In general, the ellipticities of M33
sample clusters are similar to those of M31 clusters. The structural and
dynamical parameters are derived by fitting the profiles to three different
models combined with mass-to-light ratios ($M/L$ values) from
population-synthesis models. The structural parameters include core radii,
concentration, half-light radii {\bf and} central surface brightness. The
dynamical parameters include the integrated cluster mass, integrated binding
energy, central surface mass density {\bf and} predicted line-of-sight velocity
dispersion at the cluster center. The velocity dispersions of four clusters
predicted here agree well with the observed dispersions by Larsen et al. The
results here showed that the majority of the sample halo globular clusters are
well fitted by King model as well as by Wilson model, and better than by
S\'ersic model. In general, the properties of clusters in M33, M31 and the
Milky Way fall in the same regions of parameter spaces. The tight correlations
of cluster properties indicate a "fundamental plane" for clusters, which
reflects some universal physical conditions and processes operating at the
epoch of cluster formation.
