  It is well known that for spatially flat FRW cosmologies, the holographic
dark energy disfavours the Hubble parameter as a candidate for the IR cutoff.
For overcoming this problem, we explore the use of this cutoff in holographic
ellipsoidal cosmological models, and derive the general ellipsoidal metric
induced by a such holographic energy density. Despite the drawbacks that this
cutoff presents in homogeneous and isotropic universes, based on this general
metric, we developed a suitable ellipsoidal holographic cosmological model,
filled with a dark matter and a dark energy components. At late time stages,
the cosmic evolution is dominated by a holographic anisotropic dark energy with
barotropic equations of state. The cosmologies expand in all directions in
accelerated manner. Since the ellipsoidal cosmologies given here are not
asymptotically FRW, the deviation from homogeneity and isotropy of the universe
on large cosmological scales remains constant during all cosmic evolution. This
feature allows studied holographic ellipsoidal cosmologies to be ruled by an
equation of state $\omega=p/\rho$, whose range belongs to quintessence or even
phantom matter.
