  We analyse the clustering of matter on large scales in an extension of the
concordance model that allows for spatial curvature. We develop a consistent
approach to curvature and wide-angle effects on the galaxy 2-point correlation
function in redshift space. In particular we derive the Alcock-Paczynski
distortion of $f\sigma_{8}$, which differs significantly from empirical models
in the literature. A key innovation is the use of the `Clustering Ratio', which
probes clustering in a different way to redshift-space distortions, so that
their combination delivers more powerful cosmological constraints. We use this
combination to constrain cosmological parameters, without CMB information. In a
curved Universe, we find that $\Omega_{{\rm m}, 0}=0.26\pm 0.04$ (68\% CL).
When the clustering probes are combined with low-redshift background probes --
BAO and SNIa -- we obtain a CMB-independent constraint on curvature:
$\Omega_{K,0} = 0.0041\,_{-0.0504}^{+0.0500}$. We find no Bayesian evidence
that the flat concordance model can be rejected. In addition we show that the
sound horizon at decoupling is $r_{\rm d} = 144.57 \pm 2.34 \; {\rm Mpc}$, in
agreement with its measurement from CMB anisotropies. As a consequence, the
late-time Universe is compatible with flat $\Lambda$CDM and a standard sound
horizon, leading to a small value of $H_{0}$, {\em without} assuming any CMB
information. Clustering Ratio measurements produce the only low-redshift
clustering data set that is not in disagreement with the CMB, and combining the
two data sets we obtain $\Omega_{K,0}= -0.023 \pm 0.010$.
