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[abridged] We propose a tiered, UV--near-IR, cosmological broad- andmedium-band imaging and grism survey that covers ~10 deg^2 in two epochs tom_AB=28, ~3 deg^2 in seven epochs to m_AB=28, and ~1 deg^2 in 20 epochs tom_AB=30 mag. Such a survey is an essential complement to JWST surveys (<~0.1deg^2 to m_AB<~31 mag at lambda>1100nm and z>~8). We aim to: (1) understand inhow galaxies formed from perturbations in the primordial density field bystudying faint Ly\alpha-emitting and Lyman-break galaxies at 5.5<~z<~8 andtrace the metal-enrichment of the IGM; (2) measure the evolution of the faintend of the galaxy luminosity function (LF) from z~8 to z~0 by mapping theramp-up of PopII star formation, (dwarf) galaxy formation and assembly, andhence, the objects that likely completed the H-reionization at z~6; (3)directly study the lambda<91.2nm escape fractions of galaxies and weak AGN fromz~4.0--2.5, when the He reionization finished; (4) measure the mass- andenvironment-dependent galaxy assembly process from z~5 to z~0, combiningaccurate (sigma_z/(1+z) <~ 0.02) photo-z's with spatially resolved stellarpopulations and kpc-scale structure for >~5x10^6 galaxies; (5) trace thestrongly epoch-dependent galaxy merger rate and constrain how Dark Energyaffected galaxy assembly and the growth of SMBHs; (6) study >~10^5 weakAGN/feeding SMBHs in the faint-end of the QSO LF, over 10 deg^2 and measure howthe growth of SMBHs kept pace with galaxy assembly and spheroid growth, and howthis process was shaped by various feedback processes over cosmic times sincez~8. The proposed study is not feasible with current instrumentation but arguesfor a wide-field (>~250 arcmin^2), high-resolution (<~0.02--0.11 [300--1700nm]), UV--near-IR imaging facility on a 4m-class space observatory.

Galaxy Assembly and SMBH/AGN-growth from Cosmic Dawn to the End of Reionization