  The description of spacetime is an fundamental problem of cosmology. We
explain why the current assignments of spacetime geometries for $\Omega_k$ of
the Friedmann-Lema\^{\i}tre-Robertson-Walker (FLRW) model are probably
incorrect and suggest more useful descriptions. We show that $\Omega_k$
represents not only curvature but the influence of matter density on the extent
of spacetime between massive objects. Recent analyses of supernovae type Ia
(SNe Ia) and HII/GEHR data with the FLRW model present the best fits with a
small value for $\Omega_m$ and a large $\Omega_k$. These results are consistent
with our Universe exhibiting sparse matter density and quasi-Euclidean geometry
and the small $\Omega_m$ value agrees with Big Bang nucleosynthesis
calculations. We suggest the geometry of our current Universe is better
described by a value for $\Omega_k\approx$1 rather than 0. As an example we
extend the FLRW model towards the Big Bang and discover a simple explanation of
how matter creation developed into the currently geometrically flat Universe
with sparse, homogeneous, isotropic matter and energy distributions. Assigning
$\Omega_k\approx1$ to describe quasi-Euclidean spacetime geometry is also
useful for estimating $H_0$ and should help resolve the tension surrounding
current estimates by different investigators.
