We present electro-photometric UBV and high-speed U-band flickering observations of the recurrent nova T CrB during a period when its U brightness varies by more than 2 mag. The V band is dominated by the ellipsoidal variability of the red giant; however, the variability of the hot component also causes ∼0.15-mag variations in V. We define a set of parameters that characterize the flickering. The Fourier spectra of all 27 nights are similar to each other. The power spectral density of the variations has a power-law component (∝f–1.46 on average). We do not detect a dependence of the Fourier spectra and autocorrelation function on the brightness of the object. Having subtracted the contribution of the red giant, we show that the flickering amplitude correlates with the average flux of the accreting component. A comparison with CH Cyg and MWC 560 indicates that the flickering of T CrB is more stable (at least during the time of our observations) than that in these jet-ejecting symbiotic stars. The data are available in electronic form from the authors.