  By way of a complete integration of the Friedmann equations, in terms of
observables, it is shown that for the cosmological constant $\Lambda > 0$ there
exist non-flat FLRW models for which the total density parameter $\Omega$
remains $\sim 1$ throughout the entire history of the universe. Further, it is
shown that in a precise quantitative sense these models are not finely tuned.
When observations are brought to bear on the theory, and in particular the WMAP
observations, they confirm that we live in just such a universe. The conclusion
holds when the classical notion of $\Lambda$ is extended to dark energy.
